Taxa de câmbio e composição setorial da produção : sintomas de desindustrialização da economia brasileira

A participação da indústria de transformação no PIB brasileiro vem declinando desde oinício da década de 80, e esta tendência vem se acentuando juntamente com a apreciação da taxa decâmbio observada nos últimos anos. Neste artigo analisamos este processo de desindustrialização,enfatizando a influência de tal apreciação e da balança comercial. Apesar de a produção industrialestar crescendo, observa-se uma redução da sua participação relativa na pauta de exportações e novalor adicionado da economia. Dado o vigor da demanda doméstica, o efeito negativo da apreciaçãocambial é de difícil identificação. A inovação deste trabalho reside na análise mais detalhada dosdados setoriais de forma a identificar padrões de transformação da produção que são imperceptíveisquando observados pela ótica da produção agregada.

The supermassive black hole in the Seyfert 2 galaxy NGC 5252

We present results from HST/STIS long-slit spectroscopy of the gas motions in the nuclear region of the Seyfert 2 galaxy NGC 5252. The observed velocity field is consistent with gas in regular rotation with superposed localized patches of disturbed gas. The dynamics of the circumnuclear gas can be accurately reproduced by adding to the stellar mass component a compact dark mass of MBH = 0.95 (-0.45;+1.45) 10E9 M(sun), very likely a supermassive black hole. Contrarily to results obtained in similar studies rotational broadening is sufficient to reproduce also the behaviour of line widths. The MBH estimated for NGC 5252 is in good agreement with the correlation between MBH and bulge mass. The comparison with the MBH vs sigma relationship is less stringent (mostly due to the relatively large error in sigma); NGC 5252 is located above the best fit line by between 0.3 and 1.2 dex, i.e. 1 - 4 times the dispersion of the correlation. Both the galaxy's and MBH of NGC 5252 are substantially larger than those usually estimated for Seyfert galaxies but, on the other hand, they are typical of radio-quiet quasars. Combining the determined MBH with the hard X-ray luminosity, we estimate that NGC 5252 is emitting at a fraction ~ 0.005 of L(Edd). In this sense, this active nucleus appears to be a quasar relic, now probably accreting at a low rate, rather than a low black hole mass counterpart of a QSO.Comment: Accepted for publication in A&

Teses equivocadas no debate sobre desindustrialização e perda de competitividade da indústria brasileira

O presente artigo tem por objetivo apresentar as teses da ortodoxia sobre a desindustrialização da economia brasileira, apontando a razão pela qual as mesmas são equivocadas. Como iremos argumentar ao longo deste artigo, a desindustrialização brasileira não é uma decorrência natural do processo de desenvolvimento, sendo de natureza precoce e causada, sobretudo, pela apreciação cambial decorrente da valorização dos termos de troca observada nos últimos anos. Além disso, a desindustrialização não é um fenômeno irrelevante sobre o desenvolvimento da economia brasileira no médio e longo-prazo, uma vez que a indústria não é um setor como outro qualquer, mas é o setor onde se observam os maiores níveis da produtividade do trabalho

Low Surface Brightness Galaxies in the SDSS: the link between environment, star-forming properties and AGN

Using the Sloan Digital Sky Survey (SDSS) data release 4 (DR 4), we investigate the spatial distribution of low and high surface brightness galaxies (LSBGs and HSBGs, respectively). In particular, we focus our attention on the influence of interactions between galaxies on the star formation strength in the redshift range $0.01 < z < 0.1$. With cylinder counts and projected distance to the first and fifth-nearest neighbor as environment tracers, we find that LSBGs tend to have a lack of companions compared to HSBGs at small scales ($<2$ Mpc). Regarding the interactions, we have evidence that the fraction of LSBGs with strong star formation activity increases when the distance between pairs of galaxies ($r_{p}$) is smaller than about four times the Petrosian radius ($r_{90}$) of one of the components. Our results suggest that, rather than being a condition for their formation, the isolation of LSBGs is more connected with their survival and evolution. The effect of the interaction on the star formation strength, measured by the average value of the birthrate parameter $b$, seems to be stronger for HSBGs than for LSBGs. The analysis of our population of LSBGs and HSBGs hosting an AGN show that, regardless of the mass range, the fraction of LSBGs having an AGN is lower than the corresponding fraction of HSBGs with an AGN. Also, we observe that the fraction of HSBGs and LSBGs having an AGN increases with the bulge luminosity. These results, and those concerning the star-forming properties of LSBGs as a function of the environment, fit with the scenario proposed by some authors where, below a given threshold of surface mass density, low surface brightness disks are unable to propagate instabilities, preventing the formation and evolution of massive black holes in the centers of LSBGs.Comment: 33 pages, 13 Figures, 2 Tables. Accepted for publication in The Astrophysical Journal (January 2011 Issue

An Alternative Approach To Measuring Reverberation Lags in Active Galactic Nuclei

Motivated by recent progress in the statistical modeling of quasar variability, we develop a new approach to measuring emission-line reverberation lags to estimate the size of broad-line regions (BLRs) in active galactic nuclei. Assuming that all emission-line light curves are scaled, smoothed, and displaced versions of the continuum, this alternative approach fits the light curves directly using a damped random walk model and aligns them to recover the time lag and its statistical confidence limits. We introduce the mathematical formalism of this approach and demonstrate its ability to cope with some of the problems for traditional methods, such as irregular sampling, correlated errors, and seasonal gaps. We redetermine the lags for 87 emission lines in 31 quasars and reassess the BLR size--luminosity relationship using 60 H-beta lags. We confirm the general results from the traditional cross-correlation methods, with a few exceptions. Our method, however, also supports a broad range of extensions. In particular, it can simultaneously fit multiple lines and continuum light curves which improves the lag estimate for the lines and provides estimates of the error correlations between them. Determining these correlations is of particular importance for interpreting emission-line velocity--delay maps. We can also include parameters for luminosity-dependent lags or line responses. We use this to detect the scaling of the BLR size with continuum luminosity in NGC 5548.Comment: match to the version accepted to ApJ. New code release available at http://www.astronomy.ohio-state.edu/~yingzu/spear.htm

A note on black hole masses estimated by the second moment in Narrow Line Seyfert 1 Galaxies

The second moment of the H$\beta$ emission line is calculated for 329 narrow line Seyfert 1 galaxies (NLS1s) selected from the Sloan Digital Sky Survey (SDSS), which is used to calculate the central supermassive black hole (SMBHs) mass of each. We find that the second moment depends strongly on the broader component of the H$\beta$ line profile. We find that for the NLS1s requiring two Gaussians to fit the H$\beta$ line the mean value of the SMBH mass from the H$\beta$ second moment is larger by about 0.50 dex than that from the full width at half maximum (FWHM). Using the gas velocity dispersion of the core/narrow component of \oiii $\lambda$ 5007 to estimate the stellar velocity dispersion, $\sigma_{*}$, the new mass makes NLS1s fall very close to the \mbh - \sigma_{*} relation for normal AGNs. By using $\sigma_{*}$ measured directly from SDSS spectra with a simple stellar population synthesis method, we find that for NLS1s with mass lower than 10^7 \msun, they fall only marginally below the \mbh - \sigma_{*} relation considering the large scatter in the mass calculation.Comment: 8 paper, 5 figures, 1 tables, accepted for publication in MNRA